Cold prominence materials detected within magnetic clouds during 1998–2007

Wang, Jiemin; Feng, H. Q.; Zhao, Guoqing

doi:10.1051/0004-6361/201731807

Cited by 16 publications

(24 citation statements)

References 37 publications

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“…The work reported that magnetic clouds exhibit higher ionic charge states than non-magnetic clouds. In addition, statistical results demonstrated that fast magnetic clouds have higher charge states and relative elemental abundances (except the C/O) than slow ones (Owens, 2018;Huang et al, 2020), and cold prominence plasmas with lower charge states can be detected within ICMEs near 1 au (Lepri and Zurbuchen, 2010;Gilbert et al, 2012;Sharma and Srivastava, 2012;Wang, Feng, and Zhao, 2018;Feng et al, 2018). Zurbuchen et al (2016) performed a comprehensive analysis of the elemental abundances of 310 ICMEs on Richardson and Cane's catalog from 1998 March to 2011 August (Richardson and Cane, 2010).…”

Section: Introductionmentioning

confidence: 99%

Solar Cycle Dependence of ICME Composition

Song

Sun

et al. 2021

Sol Phys

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Coronal mass ejections (CMEs) belong to the most energetic explosions in the solar atmosphere, and their occurrence rates exhibit obvious solar cycle dependence with more events taking place around solar maximum. Composition of interplanetary CMEs (ICMEs), referring to the charge states and elemental abundances of ions, opens an important avenue to investigate CMEs. In this paper, we conduct a statistical study on the charge states of five elements (Mg, Fe, Si, C, and O) and the relative abundances of six elements (Mg/O, Fe/O, Si/O, C/O, Ne/O, and He/O) within ICMEs from 1998 to 2011, and find that all the ICME compositions possess a solar cycle dependence. All of the ionic charge states and most of the relative elemental abundances are positively correlated with sunspot numbers (SSNs), and only the C/O ratios are inversely correlated with the SSNs. The compositions (except the C/O) increase with the SSNs during the ascending phase (1998–2000 and 2009–2011) and remain elevated during solar maximum and descending phase (2000–2005) compared to solar minimum (2007–2009). The charge states of low-FIP (first ionization potential) elements (Mg, Fe, and Si) and their relative abundances are correlated well, while no clear correlation is observed between the C6+/C5+ or C6+/C4+ and C/O. Most interestingly, we find that the Ne/O ratios of ICMEs and slow solar wind have the opposite solar cycle dependence.

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Section: Introductionmentioning

confidence: 99%

Solar Cycle Dependence of ICME Composition

Song

Sun

et al. 2021

Sol Phys

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“…Hence, the predicted observational characteristics of interplanetary remnant prominence materials should have low temperature, high density, and low ionic charge states, and these signatures can be taken as evidence to identify prominence material. However, the observational low temperature and high density characteristics can be modified by propagation effects when solar wind flows propagate from the Sun to the Earth (Janvier et al 2014;Wang et al 2018). The new high-density regions can be formed, and original low-temperature regions also can disappear near 1 AU through the non-uniform expansion of magnetic structures in the solar wind (Wang et al 2018).…”

Section: Methodsmentioning

confidence: 99%

“…However, the observational low temperature and high density characteristics can be modified by propagation effects when solar wind flows propagate from the Sun to the Earth (Janvier et al 2014;Wang et al 2018). The new high-density regions can be formed, and original low-temperature regions also can disappear near 1 AU through the non-uniform expansion of magnetic structures in the solar wind (Wang et al 2018). The ionic charge states in the interplanetary media mainly depend on their solar source temperature because the solar wind ion charge states are nearly frozen near the Sun (Heidrich-Meisner et al 2016;Wang & Feng 2016;Wang et al 2018).…”

Section: Methodsmentioning

confidence: 99%

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Possible Cool Prominence Materials Detected within Interplanetary Small Magnetic Flux Ropes

Wang

Feng

et al. 2019

ApJ

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Previous studies indicate that interplanetary small magnetic flux ropes (SMFRs) are manifestations of microflare-associated small coronal mass ejections (CMEs), and the hot material with high charge states heated by related microflares are found in SMFRs. Ordinary CMEs are frequently associated with prominence eruptions, and cool prominence materials are found within some magnetic clouds (MCs). Therefore, the predicted small CMEs may also be frequently associated with small prominence eruptions. In this work, we aim to search for cool prominence materials within SMFRs. We examined all the O 5+ and Fe 6+ fraction data obtained by the Advanced Composition Explorer spacecraft during 1998 to 2008 and found that 13 SMFRs might exhibit low-charge-state signatures of unusual O 5+ and/or Fe 6+ abundances. One of the 13 SMFRs also exhibited signatures of high ionic charge states. We also reported a SMFR with high Fe 6+ fraction, but the values of Fe 6+ is a little lower than the threshold defining unusual Fe 6+ . However, the SDO/AIA observations confirmed that the progenitor CME of this SMFR is associated with a small eruptive prominence, and the observations also supported the prominence materials were embedded in the CME. These observations are at the edge of the capabilities of ACE/SWICS and it cannot be ruled out that they are solely caused by instrumental effects. If these observations are real, they provide new evidence for the conjecture that SMFRs are small-scale MCs but also imply that the connected small CMEs could be associated with flares and prominence eruptions.

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“…In some cases, eruptive prominences can be traced into the upper corona to become CME bright cores (House et al, 1981;Illing & Athay, 1986;Gopalswamy et al, 1998). Cold material evidently belonging to remnants of eruptive filaments is also detected within interplanetary CMEs (ICMEs), which are interplanetary manifestations of CMEs (Lepri & Zurbuchen, 2010;Wang et al, 2018).…”

Section: Introductionmentioning

confidence: 99%

Difference of source regions between fast and slow coronal mass ejections

Filippov

2019

Publ. Astron. Soc. Aust.

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Coronal mass ejections (CMEs) are tightly related to filament eruptions and usually are their continuation in the upper solar corona. It is common practice to divide all observed CMEs into fast and slow ones. Fast CMEs usually follow eruptive events in active regions near big sunspot groups and associated with major solar flares. Slow CMEs are more related to eruptions of quiescent prominences located far from active regions. We analyze ten eruptive events with particular attention to the events on 2013 September 29 and on 2016 January 26, one of which was associated with a fast CME, while another was followed by a slow CME. We estimated the initial store of free magnetic energy in the two regions and show the resemblance of pre-eruptive situations. The difference of late behaviour of the two eruptive prominences is a consequence of the different structure of magnetic field above the filaments. We estimated this structure on the basis of potential magnetic field calculations. Analysis of other eight events confirmed that all fast CMEs originate in regions with rapidly changing with height value and direction of coronal magnetic field.

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Cold prominence materials detected within magnetic clouds during 1998–2007

Cited by 16 publications

References 37 publications

Solar Cycle Dependence of ICME Composition

Solar Cycle Dependence of ICME Composition

Possible Cool Prominence Materials Detected within Interplanetary Small Magnetic Flux Ropes

Difference of source regions between fast and slow coronal mass ejections

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